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1. Clustering of CODEX clusters

Author

Lindholm, Valtteri, Finoguenov, Alexis, Comparat, Johan, Kirkpatrick, Charles C., Rykoff, Eli, Clerc, Nicolas, Collins, Chris, Damsted, Sanna, Chitham, Jacob Ider, and Padilla, Nelson

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aims. We analyze the autocorrelation function of a large contiguous sample of galaxy clusters, the Constrain Dark Energy with X-ray (CODEX) sample, in which we take particular care of cluster definition. These clusters were X-ray selected using the RASS survey and then identified as galaxy clusters using the code redMaPPer run on the photometry of the SDSS. We develop methods for precisely accounting for the sample selection effects on the clustering and demonstrate their robustness using numerical simulations. Methods. Using the clean CODEX sample, which was obtained by applying a redshift-dependent richness selection, we computed the two-point autocorrelation function of galaxy clusters in the $0.1

Published
2020
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2. Exploring cosmic origins with CORE: gravitational lensing of the CMB

Author

Challinor, Anthony, Allison, Rupert, Carron, Julien, Errard, Josquin, Feeney, Stephen, Kitching, Thomas, Lesgourgues, Julien, Lewis, Antony, Zubeldía, Íñigo, Achucarro, Ana, Ade, Peter, Ashdown, Mark, Ballardini, Mario, Banday, A. J., Banerji, Ranajoy, Bartlett, James, Bartolo, Nicola, Basak, Soumen, Baumann, Daniel, Bersanelli, Marco, Bonaldi, Anna, Bonato, Matteo, Borrill, Julian, Bouchet, François, Boulanger, François, Brinckmann, Thejs, Bucher, Martin, Burigana, Carlo, Buzzelli, Alessandro, Cai, Zhen-Yi, Calvo, Martino, Carvalho, Carla-Sofia, Castellano, Gabriella, Chluba, Jens, Clesse, Sebastien, Colantoni, Ivan, Coppolecchia, Alessandro, Crook, Martin, d'Alessandro, Giuseppe, de Bernardis, Paolo, de Gasperis, Giancarlo, De Zotti, Gianfranco, Delabrouille, Jacques, Di Valentino, Eleonora, Diego, Jose-Maria, Fernandez-Cobos, Raul, Ferraro, Simone, Finelli, Fabio, Forastieri, Francesco, Galli, Silvia, Genova-Santos, Ricardo, Gerbino, Martina, González-Nuevo, Joaquin, Grandis, Sebastian, Greenslade, Joshua, Hagstotz, Steffen, Hanany, Shaul, Handley, Will, Hernandez-Monteagudo, Carlos, Hervías-Caimapo, Carlos, Hills, Matthew, Hivon, Eric, Kiiveri, Kimmo, Kisner, Ted, Kunz, Martin, Kurki-Suonio, Hannu, Lamagna, Luca, Lasenby, Anthony, Lattanzi, Massimiliano, Liguori, Michele, Lindholm, Valtteri, López-Caniego, Marcos, Luzzi, Gemma, Maffei, Bruno, Martinez-González, Enrique, Martins, C. J. A. P., Masi, Silvia, McCarthy, Darragh, Melchiorri, Alessandro, Melin, Jean-Baptiste, Molinari, Diego, Monfardini, Alessandro, Natoli, Paolo, Negrello, Mattia, Notari, Alessio, Paiella, Alessandro, Paoletti, Daniela, Patanchon, Guillaume, Piat, Michel, Pisano, Giampaolo, Polastri, Linda, Polenta, Gianluca, Pollo, Agnieszka, Poulin, Vivian, Quartin, Miguel, Remazeilles, Mathieu, Roman, Matthieu, Rubino-Martin, Jose-Alberto, Salvati, Laura, Tartari, Andrea, Tomasi, Maurizio, Tramonte, Denis, Trappe, Neil, Trombetti, Tiziana, Tucker, Carole, Valiviita, Jussi, Van de Weijgaert, Rien, van Tent, Bartjan, Vennin, Vincent, Vielva, Patricio, Vittorio, Nicola, Young, Karl, and Zannoni, Mario

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Lensing of the CMB is now a well-developed probe of large-scale clustering over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission can produce a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that it will enable. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous BAO measurements, three times smaller than the minimum total mass allowed by neutrino oscillations. In the search for B-mode polarization from primordial gravitational waves with CORE, lens-induced B-modes will dominate over instrument noise, limiting constraints on the gravitational wave power spectrum amplitude. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60%. This improves to 70% by combining lensing and CIB measurements from CORE, reducing the error on the gravitational wave amplitude by 2.5 compared to no delensing (in the null hypothesis). Lensing measurements from CORE will allow calibration of the halo masses of the 40000 galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. CORE can accurately remove Galactic emission from CMB maps with its 19 frequency channels. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE. [abridged], Comment: 44 pages, 12 figures

Published
2017
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3. Exploring Cosmic Origins with CORE: Inflation

Author

CORE Collaboration, Finelli, Fabio, Bucher, Martin, Achúcarro, Ana, Ballardini, Mario, Bartolo, Nicola, Baumann, Daniel, Clesse, Sébastien, Errard, Josquin, Handley, Will, Hindmarsh, Mark, Kiiveri, Kimmo, Kunz, Martin, Lasenby, Anthony, Liguori, Michele, Paoletti, Daniela, Ringeval, Christophe, Väliviita, Jussi, van Tent, Bartjan, Vennin, Vincent, Allison, Rupert, Arroja, Frederico, Ashdown, Marc, Banday, A. J., Banerji, Ranajoy, Bartlett, James G., Basak, Soumen, Baselmans, Jochem, de Bernardis, Paolo, Bersanelli, Marco, Bonaldi, Anna, Borril, Julian, Bouchet, François R., Boulanger, François, Brinckmann, Thejs, Burigana, Carlo, Buzzelli, Alessandro, Cai, Zhen-Yi, Calvo, Martino, Carvalho, Carla Sofia, Castellano, Gabriella, Challinor, Anthony, Chluba, Jens, Colantoni, Ivan, Crook, Martin, D'Alessandro, Giuseppe, D'Amico, Guido, Delabrouille, Jacques, Desjacques, Vincent, De Zotti, Gianfranco, Diego, Jose Maria, Di Valentino, Eleonora, Feeney, Stephen, Fergusson, James R., Fernandez-Cobos, Raul, Ferraro, Simone, Forastieri, Francesco, Galli, Silvia, García-Bellido, Juan, de Gasperis, Giancarlo, Génova-Santos, Ricardo T., Gerbino, Martina, González-Nuevo, Joaquin, Grandis, Sebastian, Greenslade, Josh, Hagstotz, Steffen, Hanany, Shaul, Hazra, Dhiraj K., Hernández-Monteagudo, Carlos, Hervias-Caimapo, Carlos, Hills, Matthew, Hivon, Eric, Hu, Bin, Kisner, Ted, Kitching, Thomas, Kovetz, Ely D., Kurki-Suonio, Hannu, Lamagna, Luca, Lattanzi, Massimiliano, Lesgourgues, Julien, Lewis, Antony, Lindholm, Valtteri, Lizarraga, Joanes, López-Caniego, Marcos, Luzzi, Gemma, Maffei, Bruno, Mandolesi, Nazzareno, Martínez-González, Enrique, Martins, Carlos J. A. P., Masi, Silvia, McCarthy, Darragh, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Molinari, Diego, Monfardini, Alessandro, Natoli, Paolo, Negrello, Mattia, Notari, Alessio, Oppizzi, Filippo, Paiella, Alessandro, Pajer, Enrico, Patanchon, Guillaume, Patil, Subodh P., Piat, Michael, Pisano, Giampaolo, Polastri, Linda, Polenta, Gianluca, Pollo, Agnieszka, Poulin, Vivian, Quartin, Miguel, Ravenni, Andrea, Remazeilles, Mathieu, Renzi, Alessandro, Roest, Diederik, Roman, Matthieu, Rubiño-Martin, Jose Alberto, Salvati, Laura, Starobinsky, Alexei A., Tartari, Andrea, Tasinato, Gianmassimo, Tomasi, Maurizio, Torrado, Jesús, Trappe, Neil, Trombetti, Tiziana, Tucker, Carole, Tucci, Marco, Urrestilla, Jon, van de Weygaert, Rien, Vielva, Patricio, Vittorio, Nicola, and Young, Karl

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We forecast the scientific capabilities to improve our understanding of cosmic inflation of CORE, a proposed CMB space satellite submitted in response to the ESA fifth call for a medium-size mission opportunity. The CORE satellite will map the CMB anisotropies in temperature and polarization in 19 frequency channels spanning the range 60-600 GHz. CORE will have an aggregate noise sensitivity of $1.7 \mu$K$\cdot \,$arcmin and an angular resolution of 5' at 200 GHz. We explore the impact of telescope size and noise sensitivity on the inflation science return by making forecasts for several instrumental configurations. This study assumes that the lower and higher frequency channels suffice to remove foreground contaminations and complements other related studies of component separation and systematic effects, which will be reported in other papers of the series "Exploring Cosmic Origins with CORE." We forecast the capability to determine key inflationary parameters, to lower the detection limit for the tensor-to-scalar ratio down to the $10^{-3}$ level, to chart the landscape of single field slow-roll inflationary models, to constrain the epoch of reheating, thus connecting inflation to the standard radiation-matter dominated Big Bang era, to reconstruct the primordial power spectrum, to constrain the contribution from isocurvature perturbations to the $10^{-3}$ level, to improve constraints on the cosmic string tension to a level below the presumptive GUT scale, and to improve the current measurements of primordial non-Gaussianities down to the $f_{NL}^{\rm local} < 1$ level. For all the models explored, CORE alone will improve significantly on the present constraints on the physics of inflation. Its capabilities will be further enhanced by combining with complementary future cosmological observations., Comment: Latex 107 pages, revised with updated author list and minor modifications

Published
2016
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4. Exploring Cosmic Origins with CORE: Cosmological Parameters

Author

Di Valentino, Eleonora, Brinckmann, Thejs, Gerbino, Martina, Poulin, Vivian, Bouchet, François R., Lesgourgues, Julien, Melchiorri, Alessandro, Chluba, Jens, Clesse, Sebastien, Delabrouille, Jacques, Dvorkin, Cora, Forastieri, Francesco, Galli, Silvia, Hooper, Deanna C., Lattanzi, Massimiliano, Martins, Carlos J. A. P., Salvati, Laura, Cabass, Giovanni, Caputo, Andrea, Giusarma, Elena, Hivon, Eric, Natoli, Paolo, Pagano, Luca, Paradiso, Simone, Rubino-Martin, Jose Alberto, Achucarro, Ana, Ade, Peter, Allison, Rupert, Arroja, Frederico, Ashdown, Marc, Ballardini, Mario, Banday, A. J., Banerji, Ranajoy, Bartolo, Nicola, Bartlett, James G., Basak, Soumen, Baselmans, Jochem, Baumann, Daniel, de Bernardis, Paolo, Bersanelli, Marco, Bonaldi, Anna, Bonato, Matteo, Borrill, Julian, Boulanger, François, Bucher, Martin, Burigana, Carlo, Buzzelli, Alessandro, Cai, Zhen-Yi, Calvo, Martino, Carvalho, Carla Sofia, Castellano, Gabriella, Challinor, Anthony, Charles, Ivan, Colantoni, Ivan, Coppolecchia, Alessandro, Crook, Martin, D'Alessandro, Giuseppe, De Petris, Marco, De Zotti, Gianfranco, Diego, Josè Maria, Errard, Josquin, Feeney, Stephen, Fernandez-Cobos, Raul, Ferraro, Simone, Finelli, Fabio, de Gasperis, Giancarlo, Génova-Santos, Ricardo T., González-Nuevo, Joaquin, Grandis, Sebastian, Greenslade, Josh, Hagstotz, Steffen, Hanany, Shaul, Handley, Will, Hazra, Dhiraj K., Hernández-Monteagudo, Carlos, Hervias-Caimapo, Carlos, Hills, Matthew, Kiiveri, Kimmo, Kisner, Ted, Kitching, Thomas, Kunz, Martin, Kurki-Suonio, Hannu, Lamagna, Luca, Lasenby, Anthony, Lewis, Antony, Liguori, Michele, Lindholm, Valtteri, Lopez-Caniego, Marcos, Luzzi, Gemma, Maffei, Bruno, Martin, Sylvain, Martinez-Gonzalez, Enrique, Masi, Silvia, McCarthy, Darragh, Melin, Jean-Baptiste, Mohr, Joseph J., Molinari, Diego, Monfardini, Alessandro, Negrello, Mattia, Notari, Alessio, Paiella, Alessandro, Paoletti, Daniela, Patanchon, Guillaume, Piacentini, Francesco, Piat, Michael, Pisano, Giampaolo, Polastri, Linda, Polenta, Gianluca, Pollo, Agnieszka, Quartin, Miguel, Remazeilles, Mathieu, Roman, Matthieu, Ringeval, Christophe, Tartari, Andrea, Tomasi, Maurizio, Tramonte, Denis, Trappe, Neil, Trombetti, Tiziana, Tucker, Carole, Väliviita, Jussi, van de Weygaert, Rien, Van Tent, Bartjan, Vennin, Vincent, Vermeulen, Gérard, Vielva, Patricio, Vittorio, Nicola, Young, Karl, and Zannoni, Mario

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory
Abstract

We forecast the main cosmological parameter constraints achievable with the CORE space mission which is dedicated to mapping the polarisation of the Cosmic Microwave Background (CMB). CORE was recently submitted in response to ESA's fifth call for medium-sized mission proposals (M5). Here we report the results from our pre-submission study of the impact of various instrumental options, in particular the telescope size and sensitivity level, and review the great, transformative potential of the mission as proposed. Specifically, we assess the impact on a broad range of fundamental parameters of our Universe as a function of the expected CMB characteristics, with other papers in the series focusing on controlling astrophysical and instrumental residual systematics. In this paper, we assume that only a few central CORE frequency channels are usable for our purpose, all others being devoted to the cleaning of astrophysical contaminants. On the theoretical side, we assume LCDM as our general framework and quantify the improvement provided by CORE over the current constraints from the Planck 2015 release. We also study the joint sensitivity of CORE and of future Baryon Acoustic Oscillation and Large Scale Structure experiments like DESI and Euclid. Specific constraints on the physics of inflation are presented in another paper of the series. In addition to the six parameters of the base LCDM, which describe the matter content of a spatially flat universe with adiabatic and scalar primordial fluctuations from inflation, we derive the precision achievable on parameters like those describing curvature, neutrino physics, extra light relics, primordial helium abundance, dark matter annihilation, recombination physics, variation of fundamental constants, dark energy, modified gravity, reionization and cosmic birefringence. (ABRIDGED), Comment: 90 pages, 25 Figures. Revised version with new authors list and references

Published
2016
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5. Two-Point Correlation Function as a Cosmological Probe

Author

Lindholm, Valtteri, University of Helsinki, Faculty of Science, Doctoral Programme in Particle Physics and Universe Sciences, Helsingin yliopisto, matemaattis-luonnontieteellinen tiedekunta, Alkeishiukkasfysiikan ja maailmankaikkeuden tutkimuksen tohtoriohjelma, Helsingfors universitet, matematisk-naturvetenskapliga fakulteten, Doktorandprogrammet i elementarpartikelfysik och kosmologi, Lavaux, Guilhem, Kurki-Suonio, Hannu, and Keihänen, Elina

Subjects
fysiikka
Abstract

The near-future of observational cosmology lies in extensive galaxy surveys that will map the dynamic evolution of the Universe for large part of its history. An example of such a survey is the European Space Agencys (ESA) Euclid mission. It is a space telescope scheduled to launch in 2023. The Euclid wide survey will cover 15000 square degrees, which is more than one third of the sky. It is expected to observe photometrically roughly 1.5 billion galaxies for the purposes of weak lensing analysis. In addition, 50 million galaxies will be observed spectroscopically, which will allow accurate determination of their three-dimensional distribution. The spectroscopic measurements will reach above a redshift of 2 - covering over 75% of the history of the Universe -- and photometric measurements to even higher redshifts. An important aspect of measuring the galaxy distribution is that its evolution reflects the expansion history of the Universe. It is thus a powerful tool for understanding the processes that drive the expansion. To be able to compare the evolution of the distribution with predictions from, for example, models of dark energy, we need to extract various statistics of the galaxy distribution. An important quantity is the two-point correlation function, which is a measure of amount of clustering at different spatial scales. Estimators for the two-point correlation functions rely on counting pairs of objects, usually galaxies or their clusters. The large number of galaxies Euclid is going to observe will make the clustering analysis a non-trivial computational task. The situation becomes even more challenging when one needs to estimate the covariance of the two-point correlation function estimates. This is usually done by measuring clustering of mock galaxy samples. To reach the parameter accuracy Euclid is aiming for, the number of samples needed is of the order of many thousands, thus in principle increasing the cost of a two-point correlation function estimate by the same factor. It is therefore of paramount importance to perform this analysis step as efficiently as possible. Two of the three publications included in this thesis deal with this need for efficiency. A central part of methods introduced in them is the so-called random catalog. It is a counterpart to the measured galaxy catalog that is used to model the survey geometry and various selection effects. We show that it is possible to use the random sample in clever ways to significantly speed up the computation with negligible loss of accuracy. We present one method for a single two-point correlation function estimate and another one for its covariance. We show that in a situation representative of a spectroscopic galaxy sample we can reach speed-up by a factor of order of ten -- for each method. The combined factor of hundred could already be decisive in whether the analysis is computationally feasible or not. In the end, the computational efficiency is only a tool for reaching more and more precise scientific results. The third paper in this thesis offers an example of a clustering-based cosmological analysis. Within the current theoretical understanding of the large scale structure of the Universe it is possible to obtain relations between the clustering of clusters of galaxies and the masses of their hosting dark matter halos. Generally, the more massive the halos, the more strongly clustered they are. In the paper we study this connection in detail using an X-ray selected, already-published sample of galaxy clusters. We find that the cosmological predictions for the clustering of clusters gives results that are compatible with the observations and the cosmological parameters inferred from the measurements are consistent with those obtained from the cluster mass function and the Cosmic Microwave Background. Havaitsevan kosmologian tulevaisuus on laajoissa galaksikartoituksissa, joiden avulla saadaan tarkka kuva maailmankaikkeuden laajenemishistoriasta. Yksi esimerkki tällaisesta galaksikartoitushankkeesta on Euroopan avaruusjärjestön ESA:n Euclid avaruusteleskooppi, joka laukaistaan 2023. Euclid tulee kuuden vuoden aikana kuvaamaan noin kolmanneksen taivaasta ja havainnot kattavat yli 75 % maailmankaikkeuden laajenemishistoriasta. Tämän historian puolestaan määrää maailmankaikkeuden aine-energiasisältö, mikä mahdollistaa esimerkiksi pimeän energian luonteen tutkimisen. Oleellisia ovat erilaiset galaksien avaruudellista jakaumaa kuvaavat tilastolliset suureet, joita voidaan verrata pimeän energian malleista saataviin ennusteisiin. Tärkeä esimerkki tällaisesta suureesta on galaksien kaksipistekorrelaatiofunktio, joka kuvaa galaksien klusteroitumisen voimakkuutta. Tämä funktio voidaan määrittää havaitusta galaksiaineistosta numeerisesti laskemalla galaksiparien määriä eri etäisyysskaaloilla. Esimerkiksi Euclidin tuottama suuri havaintoaineisto tekee tästä laskennallisesti raskasta. Tilanne muuttu yhä haastavammaksi, kun ryhdytään laskemaan korrelaatiofunktion hajontaa eli kovarianssia. Tämä tehdään tyypillisesti laskemalla korrelaatiofunktio suuresta määrästä, mahdollisesti useista tuhansista simuloiduista galaksikatalogeista, jolloin laskennallinen vaativuus kasvaa periaatteessa samalla kertoimella. Kaksi väitöskirjaan sisältyvästä kolmesta artikkelista pyrkii vastaamaan tähän haasteeseen tehostamalla korrelaatiofunktion ja sen kovarianssin laskemisessa käytettäviä algoritmeja. Oleellinen osa kehitettyjä menetelmiä on niin sanottu satunnaiskatalogi, jonka avulla mallinnetaan kunkin galaksikartoituksen havaitseman alueen geometriaa ja erilaisia valintaefektejä. Julkaisuissa osoitamme, että muokkaamalla satunnaiskatalogin käyttöä sopivasti voidaan sekä yksittäisen korrelaatiofunktion että sen kovarianssimatriisin määrittämiseen tarvittava laskenta-aika laskea alle kymmenesosaan tarkkuuden kärsimättä. Yhdistettynä nämä menetelmät vähentävät kovarianssin laskentavaativuutta noin tekijällä sata, mikä on ratkaisevan tärkeää esimerkiksi Euclidin data-analyysissä. Väitöskirjaan sisältyvä kolmas julkaisu on esimerkki korrelaatiofunktion käytöstä analyysissä, jossa pyritään määrittämään kosmologisen mallin parametrien arvoja. Analyysissä havaittiin, että galaksijoukkojen (jotka eivät klusteroitumisen puolesta periaatteessa eroa yksittäisistä galakseista) korrelaatiofunktiosta johdetut parametrien arvot ovat yhteensopivia esimerkiksi kosmisesta mikroaaltotaustasta saatujen tulosten kanssa.

Published
2023

6. Exploring Cosmic Origins with CORE: Cosmological Parameters

Author

Di Valentino, Eleonora, Brinckmann, Thejs, Gerbino, Martina, Poulin, Vivian, Bouchet, François R., Lesgourgues, Julien, Melchiorri, Alessandro, Chluba, Jens, Clesse, Sebastien, Delabrouille, Jacques, Dvorkin, Cora, Forastieri, Francesco, Galli, Silvia, Hooper, Deanna C., Lattanzi, Massimiliano, Martins, Carlos J. A. P., Salvati, Laura, Cabass, Giovanni, Caputo, Andrea, Giusarma, Elena, Hivon, Eric, Natoli, Paolo, Pagano, Luca, Paradiso, Simone, Rubino-Martin, Jose Alberto, Achucarro, Ana, Ade, Peter, Allison, Rupert, Arroja, Frederico, Ashdown, Marc, Ballardini, Mario, Banday, A. J., Banerji, Ranajoy, Bartolo, Nicola, Bartlett, James G., Basak, Soumen, Baselmans, Jochem, Baumann, Daniel, Bernardis, Paolo, Bersanelli, Marco, Bonaldi, Anna, Bonato, Matteo, Borrill, Julian, Boulanger, François, Bucher, Martin, Burigana, Carlo, Buzzelli, Alessandro, Cai, Zhen-Yi, Calvo, Martino, Carvalho, Carla Sofia, Castellano, Gabriella, Challinor, Anthony, Charles, Ivan, Colantoni, Ivan, Coppolecchia, Alessandro, Crook, Martin, D Alessandro, Giuseppe, Petris, Marco, Zotti, Gianfranco, Diego, Josè Maria, Errard, Josquin, Feeney, Stephen, Fernandez-Cobos, Raul, Ferraro, Simone, Finelli, Fabio, Gasperis, Giancarlo, Génova-Santos, Ricardo T., González-Nuevo, Joaquin, Grandis, Sebastian, Greenslade, Josh, Hagstotz, Steffen, Hanany, Shaul, Handley, Will, Hazra, Dhiraj K., Hernández-Monteagudo, Carlos, Hervias-Caimapo, Carlos, Hills, Matthew, Kiiveri, Kimmo, Kisner, Ted, Kitching, Thomas, Kunz, Martin, Kurki-Suonio, Hannu, Lamagna, Luca, Lasenby, Anthony, Lewis, Antony, Liguori, Michele, Lindholm, Valtteri, Lopez-Caniego, Marcos, Luzzi, Gemma, Maffei, Bruno, Martin, Sylvain, Martinez-Gonzalez, Enrique, Masi, Silvia, Mccarthy, Darragh, Melin, Jean-Baptiste, Mohr, Joseph J., Molinari, Diego, Monfardini, Alessandro, Negrello, Mattia, Notari, Alessio, Paiella, Alessandro, Paoletti, Daniela, Patanchon, Guillaume, Piacentini, Francesco, Piat, Michael, Pisano, Giampaolo, Polastri, Linda, Polenta, Gianluca, Pollo, Agnieszka, Quartin, Miguel, Remazeilles, Mathieu, Roman, Matthieu, Ringeval, Christophe, Tartari, Andrea, Tomasi, Maurizio, Tramonte, Denis, Trappe, Neil, Trombetti, Tiziana, Carole Tucker, Väliviita, Jussi, Weygaert, Rien, Tent, Bartjan, Vennin, Vincent, Vermeulen, Gérard, Vielva, Patricio, Vittorio, Nicola, Young, Karl, Zannoni, Mario, and Core, For The Collaboration

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